Attendees: Fred, Yohan, Adam, Timea, Sasha, Gemma, Allison, Hongli, Roberto, Alex, Ant, Nathalie, Amy, Fabien, Tapas
Not attending: Manuel
Minutes from our last telecon
Members and their main interests
→ to be used as a model toward which the high-resolution Tdust images should converge
Tight noise: sigma/2 for LABOCA (870) and ALMA B3 (3000); sigma/4 for ALMA B6 (1300).
Gaussian noise is assumed and levels are calculated for each map as a first step of PPMAP. These noise levels are used in the SED fit.
The effect of a non-Gaussian noise on the PPMAP results should be checked… If we were to impose some weights for the different wavelengths, PPMAP would need to be modified. → not for now!
Temperature increases from the ‘normal noise’ to ‘half noise’ and the ‘tight noise’ runs. Be careful! The “tight noise” run gives temperatures closer to that of the Herschel run.
The SED fit gets worse to the 70 micron point and a s a consequence the small heating toward MM2 is lost → the 60’’-filtering run seems more reasonable
→ The 60’’-filtering run seems better than the 30’’-filtering run
→ The ‘tight noise’ run gives temperature in the background that better corresponds to that of the Herschel run.
→ The run without B3 gives better Tdust values close to/but off the HII region.
→ Could we combine the Herschel-only map and 60’’-filtering ‘tight-noise’ map to have a continuous Tdust image? Could we fit SEDs on each pixel just dropping the negative flux?
Not discussed today